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An easily-prepared impedance matched Josephson parametric amplifier

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chinese Physics B 2021年第6期30卷 48-51页

作者： Ya-Peng Lu Quan Zuo Jia-Zheng Pan Jun-Liang Jiang Xing-Yu Wei Zi-Shuo Li Wen-Qu xu Kai-xuan Zhang Ting-Ting Guo Shuo Wang Chun-Hai Cao Wei-Wei xu Guo-Zhu Sun Pei-Heng wu Research Institute of Superconductor Electronics School of Electronic Science and EngineeringNanjing UniversityNanjing 210093China purple mountain Laboratories Nanjing 211111China

An impedance matched parametric amplifier(IMPA)with Josephson junctions is fabricated and characterized.A hybrid structure containing coplanar and strip structures is implemented to realize an impedance taper line and a plate capacitor in an LC nonlinear resonator based on Josephson *** upper plate of the capacitor is isolated with SiNx without grounding as well as the *** easily-prepared designs greatly reduce the requirements for lithography alignment and precision,which makes the fabrication process more *** experimental results show that in such IMPA a gain higher than 25 dB with a bandwidth of about 100 MHz can be *** broadband amplifier operates close to the quantum *** adjusting the working point,a higher bandwidth of about 400 MHz can be obtained with a gain of about 17 dB.

关键词： Josephson junction parametric amplification impedance matching gain and bandwidth

Implications on the origin of cosmic rays in light of 10 TV spectral softenings

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Frontiers of physics 2020年第2期15卷 101-109,F0004页

作者： Cliuan Yue Peng-Xiong Ma Qiang Yuan Yi-Zhong Fan Zhan-Fang Chen Ming-Yang Cui Hao-Ting Dai Tie-Kuang Dong Xiaoyuan Huang Wei Jiang Shi-Jun Lei Xiang Li Cheng-Ming Liu Hao Liu Yang Liu Chuan-Ning Luo xu Pan Wen-Xi Peng Rui Qiao Yi-Feng Wei Li-Bo wu Zhi-Hui xu Zun-Lei xu Guan-Wen Yuan Jing-Jing Zang Ya-Peng Zhang Yong-Jie Zhang Yun-Long Zhang Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210033China School of Astronomy and Space Science University of Science and Technology of ChinaHefei 230026China Center for High Energy Physics Peking UniversityBeijing 100871China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of ChinaHefei 230026China Key Laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China Institute of Modem Physics Chinese Academy of SciencesLanzhou 730000China

Precise measurements of the energy spectra of cosmic rays(CRs)show various kinds of features deviating from single power-laws,which give very interesting and important implications on their origin and *** measurements from a few balloon and space experiments indicate the existence of spectral softenings around 10 TV for protons(and probably also for Helium nuclei).Very recently,the DArk Matter Particle Explorer(DAMPE)measurement about the proton spectrum clearly reveals such a softening with a high *** we study the implications of these new measurements,as well as the groundbased indirect measurements,on the origin of *** find that a single component of CRs fails to fit the spectral softening and the air shower experiment data *** the framework of multiple components,we discuss two possible scenarios,the multiple source population scenario and the background plus nearby source *** scenarios give reasonable fits to the wide-band data from TeV to 100 PeV *** the anisotropy observations,the nearby source model is favored.

关键词： cosmic rays

New vacuum solar telescope and observations with high resolution

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Research in Astronomy and Astrophysics 2014年第6期14卷 705-718页

作者： Zhong Liu Jun xu Bo-Zhong Gu Sen Wang Jian-Qi You Long-Xiang Shen Ru-Wei Lu Zhen-Yu Jin Lin-Fei Chen Ke Lou Zhi Li Guang-Qian Liu Zhi xu Chang-Hui Rao Qi-Qian Hu Ru-Feng Li Hao-Wen Fu Feng Wang Men-Xian Bao Ming-Chan wu Bo-Rong Zhang Yunnan Observatories chinese academy of sciences nanjing Institute of Astronomical Optics & Technology National Astronomical ObservatoriesChinese Academy of Sciences National Astronomical Observatories Chinese Academy of Sciences purple mountain observatory Chinese Academy of Sciences Institute of Optics and Electronics Chinese Academy of Sciences Kunming University of Science and Technology

The New Vacuum Solar Telescope （NVST） is a one meter vacuum solar telescope that aims to observe fine structures on the Sun. The main goals of NVST are high resolution imaging and spectral observations, including measurements of the solar magnetic field. NVST is the primary ground-based facility used by the chinese solar research community in this solar cycle. It is located by Fuxian Lake in southwest china, where the seeing is good enough to perform high resolution observations. We first introduce the general conditions at the Fuxian Solar observatory and the primary science cases of NVST. Then, the basic structures of this telescope and instruments are described in detail. Finally, some typical high resolution data of the solar photosphere and chromosphere are also shown.

关键词： telescopes -- instrumentation: adaptive optics -- instrumentation: spec-trographs -- techniques: high angular resolution -- Sun: magnetic fields

中国科学技术大学-中国科学院紫金山天文台2.5米大视场巡天望远镜(墨子巡天望远镜)

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青海科技 2024年第1期31卷 10-24页

作者：孔旭杨戟郑宪忠王坚范璐璐娄铮朱青峰王挺贵吴雪峰薛永泉张程赵海斌蔡萍中国科学技术大学天文学系合肥230026 天文与空间科学学院中国科学技术大学南京210023 中国科学院紫金山天文台南京210023 核探测与核电子学国家重点实验室中国科学技术大学合肥230026 中国科学院光电技术研究所成都610209

中国科学技术大学-中国科学院紫金山天文台2.5米大视场巡天望远镜(即墨子巡天望远镜,WFST)是中国科学技术大学“双一流”学科平台建设项目,双方于2018年3月1日召开望远镜项目预研启动会,2019年7月正式开展望远镜建设,2023年8月望远镜建... 详细信息

中国科学技术大学-中国科学院紫金山天文台2.5米大视场巡天望远镜(即墨子巡天望远镜,WFST)是中国科学技术大学“双一流”学科平台建设项目,双方于2018年3月1日召开望远镜项目预研启动会,2019年7月正式开展望远镜建设,2023年8月望远镜建成并开展调试观测,2023年9月17日望远镜首光仪式暨科学战略研讨会召开,并成功发布仙女座星系图片,标志着望远镜设备基本达到设计标准,已经可以开展天文观测研究。墨子巡天望远镜口径2.5米,采用国际先进的主焦光学系统设计和主镜主动光学矫正技术,可实现3度视场范围内均匀高像质和极低像场畸变成像,配备7.65亿像素大靶面主焦相机,具备大视场、高像质、宽波段的特点。墨子巡天望远镜安置于青海省海西州茫崖市冷湖镇赛什腾山海拔4200米的天文台址,是冷湖天文观测基地首个投入运行并开展天文观测研究的大型设备。墨子巡天望远镜通过获取天体高精度位置和多波段亮度观测数据,监测移动天体和光变天体,高效搜寻和监测天文动态事件,可以在高能时域天文、太阳系天体普查、银河系结构和近场宇宙学等研究领域取得突破性原始创新成果。同时,墨子巡天望远镜将面向国家航天强国战略,开展太阳系近地天体等搜寻与监测研究,服务航天安全和深空探测战略需求。

关键词：光学望远镜图像巡天时域天文近地天体冷湖赛什腾山

A high dynamic range readout unit for a calorimeter

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chinese Physics C 2012年第1期36卷 71-73页

作者： ZHANG Yun-Long LI Bing FENG Chang-Qing LI Xian-Li WANG Xiao-Lian xu Zi-zong GUO Jian-Hua CAI Ming-sheng HU Yi-Ming wu Jian CHANG Jin Department of Modern Physics University of Science and Technology of ChinaHefei 230026China purple mountain observatory Nanjing 210008China

A high dynamic range readout system,consisting of a multi-dynode readout PMT and a VA32 chip,is *** LED system is set up to calibrate the relative gains between the dynodes,and the ADC counts per MIPs from dynode 7 ar... 详细信息

关键词： BGO calorimeter VA32 chip PMT LED high dynamic readout

Compact NbN resonators with high kinetic inductance

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chinese Physics B 2020年第12期29卷 107-111页

作者： Xing-Yu Wei Jia-Zheng Pan Ya-Peng Lu Jun-Liang Jiang Zi-Shuo Li Sheng Lu xue-Cou Tu Qing-Yuan Zhao Xiao-Qing Jia Lin Kang Jian Chen Chun-Hai Cao Hua-Bing Wang Wei-Wei xu Guo-Zhu Sun Pei-Heng wu Research Institute of Superconductor Electronics School of Electronic Science and EngineeringNanjing UniversityNanjing 210093China purple mountain Laboratories Nanjing 211111China

We design and fabricateλ/2 coplanar waveguide NbN resonators,the thickness and length of which are only several nanometers and hundred microns,*** quality factor of such compact resonators can reach up to 7.5×10~4 at single photon power level at 30 m K with the resonance frequency around 6.835 *** order to tune the resonant frequency,the resonator is terminated to the ground with a *** tuning the magnetic flux in the dc-SQUID,the effective inductance of the dc-SQUID is varied,which leads to the change in the resonant frequency of the *** tunability range is more than 30 MHz and the quality factor is about 3×10~*** compact and tunable NbN resonators have potential applications in the quantum information processing,such as in the precision measurement,coupling and/or reading out the quantum states of qubits.

关键词： superconducting resonator NbN kinetic inductance tunable resonator

Evidence for particle acceleration approaching PeV energies in the W51 complex

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Science Bulletin 2024年第18期69卷 2833-2841页

作者： LHAASO Collaboration Zhen Cao F.Aharonian Axikegu Y.X.Bai Y.W.Bao D.Bastieri X.J.Bi Y.J.Bi W.Bian A.V.Bukevich Q.Cao W.Y.Cao Zhe Cao J.Chang J.F.Chang A.M.Chen E.S.Chen H.X.Chen Liang Chen Lin Chen Long Chen M.J.Chen M.L.Chen Q.H.Chen S.Chen S.H.Chen S.Z.Chen T.L.Chen Y.Chen N.Cheng Y.D.Cheng M.Y.Cui S.W.Cui X.H.Cui Y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai Danzengluobu X.Q.Dong K.K.Duan J.H.Fan Y.Z.Fan J.Fang J.H.Fang K.Fang C.F.Feng H.Feng L.Feng S.H.Feng X.T.Feng Y.Feng Y.L.Feng S.Gabici B.Gao C.D.Gao Q.Gao W.Gao W.K.Gao M.M.Ge L.S.Geng G.Giacinti G.H.Gong Q.B.Gou M.H.Gu F.L.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han M.Hasan H.H.He H.N.He J.Y.He Y.He Y.K.Hor B.W.Hou C.Hou X.Hou H.B.Hu Q.Hu S.C.Hu D.H.Huang T.Q.Huang W.J.Huang X.T.Huang X.Y.Huang Y.Huang X.L.Ji H.Y.Jia K.Jia K.Jiang X.W.Jiang Z.J.Jiang M.Jin M.M.Kang I.Karpikov D.Kuleshov K.Kurinov B.B.Li C.M.Li Cheng Li Cong Li D.Li F.Li H.B.Li H.C.Li Jian Li Jie Li K.Li S.D.Li W.L.Li W.L.Li X.R.Li Xin Li Y.Z.Li Zhe Li Zhuo Li E.W.Liang Y.F.Liang S.J.Lin B.Liu C.Liu D.Liu D.B.Liu H.Liu H.D.Liu J.Liu J.L.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.Liu Y.N.Liu Q.Luo Y.Luo H.K.Lv B.Q.Ma L.L.Ma X.H.Ma J.R.Mao Z.Min W.Mitthumsiri H.J.Mu Y.C.Nan A.Neronov L.J.Ou P.Pattarakijwanich Z.Y.Pei J.C.Qi M.Y.Qi B.Q.Qiao J.J.Qin A.Raza D.Ruffolo A.Sáiz M.Saeed D.Semikoz L.Shao O.Shchegolev X.D.Sheng F.W.Shu H.C.Song Yu.V.Stenkin V.Stepanov Y.Su D.X.Sun Q.N.Sun X.N.Sun Z.B.Sun J.Takata P.H.T.Tam Q.W.Tang R.Tang Z.B.Tang W.W.Tian C.Wang C.B.Wang G.W.Wang H.G.Wang H.H.Wang J.C.Wang Kai Wang Kai Wang L.P.Wang L.Y.Wang P.H.Wang R.Wang W.Wang X.G.Wang X.Y.Wang Y.Wang Y.D.Wang Y.J.Wang Z.H.Wang Z.X.Wang Zhen Wang Zheng Wang D.M.Wei J.J.Wei Y.J.Wei T.Wen C.Y.wu H.R.wu Q.W.wu S.wu X.F.wu Y.S.wu S.Q.Xi J.Xia G.M.Xiang D.X.Xiao G.Xiao Y.L.Xin Y.Xing D.R.Xiong Z.Xiong D.L.xu R.F.xu R.X.xu W.L.xu L.xue D.H.Yan J.Z.Yan T.Yan C.W.Yang C.Y.Yang F.Yang F.F.Yang L.L.Yang M.J.Yang R.Z.Yang W.X.Yang Y.H.Yao Z.G.Yao L.Q.Yin N.Yin X.H.You Z.Y.You Y.H.Yu Q.Yuan H.Yue H.D.Zeng T.X.Zeng W.Zeng M.Zha B.B.Zhang F.Zhang H.Zhang 不详 Key Laboratory of Particle Astrophysics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of chinese academy of sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-Planck-Institut for Nuclear Physics P.O.Box 103980Heidelberg 69029Germany School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China Institute for Nuclear Research of Russian academy of sciences Moscow 117312Russia Hebei Normal University Shijiazhuang 050024China University of Science and Technology of china Hefei 230026China State Key Laboratory of Particle Detection and Electronics China Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Research Center for Astronomical Computing Zhejiang LaboratoryHangzhou 311121China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China School of Physics and Astronomy Yunnan UniversityKunming 650091China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of Physics and Astronomy(Zhuhai)&School of Physics(Guangzhou)&Sino-French Institute of Nuclear Engineering and Technology(Zhuhai) Sun Yat-sen UniversityZhuhai 519000&Guangzhou 510275GuangdongChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China APC UniversitéParis Cité

Theγ-ray emission from the W51 complex is widely acknowledged to be attributed to the interaction between the cosmic rays(CRs)accelerated by the shock of supernova remnant(SNR)W51C and the dense molecular clouds in the adjacent star-forming region,***,the maximum acceleration capability of W51C for CRs remains *** on observations conducted with the Large High Altitude Air Shower observatory(LHAASO),we report a significant detection ofγrays emanating from the W51 complex,with energies from 2 to 200 *** LHAASO measurements,for the first time,extend theγ-ray emission from the W51 complex beyond 100 TeV and reveal a significant spectrum bending at tens of *** combining the"π^(0)-decay bump"featured data from Fermi-LAT,the broadbandγ-ray spectrum of the W51 region can be well-characterized by a simple pp-collision *** observed spectral bending feature suggests an exponential cutoff at~400 TeV or a power-law break at~200 TeV in the CR proton spectrum,most likely providing the first evidence of SNRs serving as CR accelerators approaching the PeV ***,two young star clusters within W51B could also be theoretically viable to produce the most energeticγrays observed by *** findings strongly support the presence of extreme CR accelerators within the W51 complex and provide new insights into the origin of Galactic CRs.

关键词： UHE c-ray Cosmic rays SNR W51C Star clusters

Optical observations of LIGO source GW 170817 by the Antarctic Survey Telescopes at Dome A,Antarctica

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Science Bulletin 2017年第21期62卷 1433-1438页

作者： lei hu xuefeng wu igor andreoni michael c.b.ashley jeff cooke xiangqun cui fujia du zigao dai bozhong gu yi hu haiping lu xiaoyan li zhengyang li ensi liang liangduan liu bin ma zhaohui shang tianrui sun n.b.suntzeff charling tao syed a.uddin lifan wang xiaofeng wang haikun wen di xiao jin xu ji yang shihai yang xiangyan yuan hongyan zhou hui zhang jilin zhou zonghong zhu purple mountain observatory chinese academy of sciencesNanjing 210008China chinese center for antarctic astronomy Nanjing 210008China school of astronomy and space sciences university of science and technology of chinaHefei 230029China centre for astrophysics and supercomputing swinburne university of technologyHawthornVIC3122Australia the australian research council centre of excellence for gravitational wave discovery(ozgrav) Australia australian astronomical observatory north rydensw 2113Australia school of physics university of new south walesnsw 2052Australia the australian research council centre of excellence for all-sky astrophysics(caastro) Australia nanjing institute of astronomical optics and technology nanjing 210042China school of astronomy and space science and key laboratory of modern astronomy and astrophysics in ministry of education nanjing universitynanjing 210093China national astronomical observatories chinese academy of sciencesBeijing 100012China department of physics tianjin normal universitytianjin 300074china shanghai key laboratory for astrophysics shanghai normal universityshanghai 200234China george p.and cynthia woods mitchell institute for fundamental physics&astronomy texas a.&m.universitydepartment of physics and astronomy4242 tamucollege stationTX 77843USA aix marseille univ CNRS/N2P3CPPMmarseilleFrance physics department and tsinghua center for astrophysics(thca) tsinghua universityBeijing 100084China polar research institute of china shanghai 200136china department of astronomy beijing normal universitybeijing 100875china school of physics and technology wuhan universitywuhan 430072china

The LIGO detection of gravitational waves(GW) from merging black holes in 2015 marked the beginning of a new era in observational astronomy. The detection of an electromagnetic signal from a GW source is the critical next step to explore in detail the physics involved. The Antarctic Survey Telescopes(AST3),located at Dome A, Antarctica, is uniquely situated for rapid response time-domain astronomy with its continuous night-time coverage during the austral winter. We report optical observations of the GW source(GW 170817) in the nearby galaxy NGC 4993 using AST3. The data show a rapidly fading transient at around 1 day after the GW trigger, with the i-band magnitude declining from 17:23 ± 0:13 magnitude to 17:72 ± 0:09 magnitude in ~1:8 h. The brightness and time evolution of the optical transient associated with GW 170817 are broadly consistent with the predictions of models involving merging binary neutron stars. We infer from our data that the merging process ejected about ~10^(-2) solar mass of radioactive material at a speed of up to 30% the speed of light.

关键词： Gravitational waves Binary neutron stars Gamma-ray bursts

Method of Separating Cosmic-Ray Positrons from Electrons in the DAMPE Experiment

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Research in Astronomy and Astrophysics 2022年第3期22卷 115-121页

作者： Hao-Ting Dai Jing-Jing Zang Ying Wang Chuan-Ning Luo Yun-Long Zhang Zhi-Yong Zhang Yi-Feng Wei Li-Bo wu Cheng-Ming Liu Cong Zhao Xiao-Lian Wang Zi-Zong xu Guang-Shun Huang State Key Laboratory of Particle Detection and Electronics University of Science and Technology of ChinaHefei 230026China Department of Modern Physics University of Science and Technology of ChinaHefei 230026China School of Physics and Electronic Engineering Linyi UniversityLinyi 276000China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Gran Sasso Science Institute (GSSI)

A method of identifying positron/electron species from the cosmic rays was studied in the DArk Matter Particle Explorer(DAMPE)*** there is no onboard magnet on the satellite,the different features imposed by the geomagnetic field on these two species were exploited for the particle *** of this method to the simulation of on-orbit electrons/positrons/protons and the real flight data proves that separately measuring the CR positrons/electrons with DAMPE is feasible,though limited by the field of view for the present observation *** analysis on the positron flux with this method can be expected in the future.

关键词： (ISM:)cosmic rays magnetic fields (cosmology:)dark matter